Equation of state for hyperonic neutron-star matter in SU(3) flavor symmetry
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| Main Authors: | , , , |
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| Format: | Preprint |
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2025
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| _version_ | 1866912689549213696 |
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| author | Miyatsu, Tsuyoshi Cheoun, Myung-Ki Kim, Kyungsik Saito, Koichi |
| author_facet | Miyatsu, Tsuyoshi Cheoun, Myung-Ki Kim, Kyungsik Saito, Koichi |
| contents | Using a relativistic mean-field model calibrated to finite-nucleus observables and bulk properties of dense nuclear matter, we investigate hyperonic neutron-star matter within an SU(3) flavor-symmetry scheme. To retain SU(6)-based couplings within SU(3) flavor symmetry, we add a quartic $ϕ$ self-interaction and $ϕ$-$ρ$ mixing. We demonstrate the roles of $α_{v}$ ($F/(F+D)$ ratio), $θ_{v}$ (mixing angle), and $z_{v}$ (singlet-to-octet coupling ratio) in SU(3)-invariant vector-meson couplings. It is found that $z_{v}$ predominantly controls the maximum mass of a neutron star, and $2M_{\odot}$ neutron stars can be supported for $z_{v}\le0.15$. The $α_{v}$ also helps sustain large masses, whereas $θ_{v}$ has a smaller effect on neutron-star properties. This SU(3) framework reconciles nuclear and astrophysical constraints, and offers a plausible resolution to the hyperon puzzle. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2509_16559 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Equation of state for hyperonic neutron-star matter in SU(3) flavor symmetry Miyatsu, Tsuyoshi Cheoun, Myung-Ki Kim, Kyungsik Saito, Koichi Nuclear Theory High Energy Astrophysical Phenomena Nuclear Experiment Using a relativistic mean-field model calibrated to finite-nucleus observables and bulk properties of dense nuclear matter, we investigate hyperonic neutron-star matter within an SU(3) flavor-symmetry scheme. To retain SU(6)-based couplings within SU(3) flavor symmetry, we add a quartic $ϕ$ self-interaction and $ϕ$-$ρ$ mixing. We demonstrate the roles of $α_{v}$ ($F/(F+D)$ ratio), $θ_{v}$ (mixing angle), and $z_{v}$ (singlet-to-octet coupling ratio) in SU(3)-invariant vector-meson couplings. It is found that $z_{v}$ predominantly controls the maximum mass of a neutron star, and $2M_{\odot}$ neutron stars can be supported for $z_{v}\le0.15$. The $α_{v}$ also helps sustain large masses, whereas $θ_{v}$ has a smaller effect on neutron-star properties. This SU(3) framework reconciles nuclear and astrophysical constraints, and offers a plausible resolution to the hyperon puzzle. |
| title | Equation of state for hyperonic neutron-star matter in SU(3) flavor symmetry |
| topic | Nuclear Theory High Energy Astrophysical Phenomena Nuclear Experiment |
| url | https://arxiv.org/abs/2509.16559 |